The spatial distribution of DM within galaxies is unknown. However, in a number of models, the DM density is assumed to be higher near the center of galaxies as compared to the outer regions. In such models, the density profile of the DM is expressed in terms of the radial distance from the galactic center.
There are few DM density profile models [1]} based on the observed galaxy rotation curves. These include Navarro–Frenk–White (NFW)[2]}, [3]}, [4]}, Einasto[5]}, isotropic [6]} and RAR [7]}, [8]} models. Out of these, the RAR model predicts DM density near the center to be much higher as compared to the other models.
